Shell and photosphere of Sigma ORI E - New observations and improved model

Details Shell and photosphere of Sigma ORI E - New observations and improved model Shell and photosphere of Sigma ORI E - New observations and improved model

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...116...64g&link_type=abstract

Astronomy and Astrophysics, vol. 116, no. 1, Dec. 1982, p. 64-74.

Astronomy and Astrophysics

Astronomy

62

B Stars, Photosphere, Stellar Envelopes, Stellar Models, Stellar Rotation, Iue, Radial Velocity, Spaceborne Astronomy, Spectrograms, Stellar Magnetic Fields, Stellar Mass, Stellar Temperature

Scientific paper

Phase-dependent IR fluxes in the J, H, K, L, and M bands, together with visual spectrograms and IUE spectra, are used to study the helium-rich star Sigma Ori E. An effective temperature of about 22,500 K is derived, along with an angular diameter of 0.079 milliarcsec, a surface gravity of log g equals 3.85, and a mass of approximately 3 solar masses. It is shown that the star probably has not completed its pre-main-sequence contraction and is an oblique rotator with a large helium cap and two corotating clouds located almost oppositely near the intersections of the magnetic and rotational equators at a distance of 2 stellar radii.

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